145 Adeona

145 Adeona
Discovery[1]
Discovered by Christian Heinrich Friedrich Peters
Discovery date 3 June 1875
Designations
MPC designation (145) Adeona
Named after
 Adeona
Main belt, adeona family
Orbital characteristics[2][3]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 130.60 yr (47700 d)
Aphelion 3.05972 AU (457.728 Gm)
Perihelion 2.28737 AU (342.186 Gm)
2.67354 AU (399.956 Gm)
Eccentricity 0.14444
4.37 yr (1596.7 d)
18.12 km/s
233.709°
0° 13m 31.663s / day
Inclination 12.6337°
77.4206°
44.0233°
Earth MOID 1.31949 AU (197.393 Gm)
Jupiter MOID 2.13391 AU (319.228 Gm)
Jupiter Tisserand parameter 3.330
Physical characteristics
Dimensions 151.14±3.2 km[3]
149.50 ± 5.45 km[4]
Mass (2.08 ± 0.57) × 1018 kg[4]
Mean density
 1.18 ± 0.34 g/cm3[4]
Equatorial surface gravity
 0.0422 m/s²
Equatorial escape velocity
 0.0799 km/s
15.071 h (0.6280 d)
0.0433±0.002[3]
0.0467 ± 0.0116[5]
Temperature ~170 K
C (Tholen)[5]
8.13,[3] 8.050[5]

    145 Adeona is a rather large main-belt asteroid. Its surface is very dark,[5] and, based upon its classification as a C-type asteroid, is probably composed of primitive carbonaceous material. The Adeona family of asteroids is named after it.

    It was discovered by C. H. F. Peters on June 3, 1875, from the observatory at Hamilton College, Clinton, New York. Peters named it after Adeona, the Roman goddess of homecoming, because he had recently returned from a journey across the world to observe the transit of Venus. Peters also discovered 144 Vibilia on the same night.[6]

    During 2001, 145 Adeona was observed by radar from the Arecibo Observatory. The return signal matched an effective diameter of 151 ± 18 km. This is consistent with the asteroid dimensions computed through other means.[7]

    Two stellar occultations by Adeona have been observed: The first one on July 9, 2002 when it occulted an 11.8 mag star, and then again on February 3, 2005 when several observers in Japan recorded the occultation of a 10.4 mag star. The latter was consistent with a diameter of 151 km.[8][9][10]

    The Dawn mission team discussed performing a flyby of this object, however NASA decided against it in July 2016.[11] At the time this was considered Dawn was orbiting the large asteroid/dwarf planet 1 Ceres, and went on studying that body later that year.[12] Dawn had previously orbited asteroid 4 Vesta, before traveling to Ceres.[12]

    See also

    References

    1. ↑
    2. ↑ "The Asteroid Orbital Elements Database". astorb. Lowell Observatory.
    3. 1 2 3 4 "145 Adeona". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 12 May 2016.
    4. 1 2 3 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73, pp. 98–118, Bibcode:2012P&SS...73...98C, arXiv:1203.4336 Freely accessible, doi:10.1016/j.pss.2012.03.009.
    5. 1 2 3 4 Pravec, P.; et al. (May 2012), "Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations", Asteroids, Comets, Meteors 2012, Proceedings of the conference held May 16–20, 2012 in Niigata, Japan (1667), Bibcode:2012LPICo1667.6089P.
    6. ↑ Lutz D. Schmadel, Dictionary of Minor Planet Names, p.28.
    7. ↑ Magri, Christopher; et al. (January 2007), "A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003", Icarus, 186 (1): 126–151, Bibcode:2007Icar..186..126M, doi:10.1016/j.icarus.2006.08.018
    8. ↑ "OBSERVED MINOR PLANET OCCULTATION EVENTS". David Dunham. July 26, 2005. Retrieved June 3, 2017.
    9. ↑ "Results of Asteroidal occultation". Sendai Space Hall. Retrieved June 3, 2017.
    10. ↑ "Occultation of (145) Adeona on 2005.2.3". Sendai Space Hall. Retrieved June 3, 2017.
    11. ↑ http://www.nasa.gov/feature/new-horizons-receives-mission-extension-to-kuiper-belt-dawn-to-remain-at-ceres
    12. 1 2 Landau, Elizabeth (November 18, 2016). "New Ceres Views as Dawn Moves Higher". NASA / Jet Propulsion Laboratory. Retrieved November 20, 2016.


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